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Massive Galaxies, Tucson Nov 1st 2006

Diagnostics of Feedback & Environmental Processes in the Evolution of Cluster & Field Galaxies. Richard Ellis Caltech. Massive Galaxies, Tucson Nov 1st 2006.

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Massive Galaxies, Tucson Nov 1st 2006

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  1. Diagnostics of Feedback & Environmental Processes in the Evolution of Cluster & Field Galaxies Richard Ellis Caltech Massive Galaxies, Tucson Nov 1st 2006

  2. In understanding evolution of massive galaxies, need to distinguish between, and relate, galactic-scale `feedback’ and externally-driven environmental processes: both are important • Major questions: • - mass & environmental dependence of SF & assembly - what limits growth of massive galaxies? - origin of morphology-density relation: nature of S0s • Detailed studies of z < 1 field & rich clusters important • Resolved dynamical studies play a unique role Key Issues With: Sean Moran, Lauren MacArthur (Caltech), Kevin Bundy (Toronto), Tommaso Treu (UCSB), Pieter van Dokkum (Yale) + DEEP2 team

  3. Mass fn:  (M, ) f() Fraction in red light Importance of Environment:  (Mpc-2) ~25% of all stars at z~0 are in ellipticals (75% in spheroids) Most are in massive galaxies whose mass function is correlated with 25% of stellar mass is in dense environments (lg  > 0.4) Baldry et al (astro-ph/0607648)

  4. Evolution of Morphology Density Relation Smith et al Ap J 620, 78 (2005) fE/S0 fE/S0 Environmental density  plays key role in governing morphological mix: - Continued growth in high  but delay for lower  regions - Slower conversion of spirals to S0s with only Es at z > 1?

  5. Applications at intermediate z: • Spheroidal galaxies: FP yields M/L ratios of field & cluster galaxies as function of mass, environmental density and redshift. Can compare dynamical and stellar masses and determine growth rates • Disk galaxies: Scatter on TF relation can test effects of environment • (in progress..) • Es vs S0s: Absorption line rotation curves can provide a more robust dynamical distinction c.f. morphology • Bulges: FP can define mass growth rate (c.f. AGN) Dynamical Studies of z<1 Galaxies All relevant in quantifying environmental & feedback effects

  6. Lensing & Dynamical Masses Correlate Well (aper = re/8) (SDSS aper = 3”) SIE derived from singular isothermal ellipsoid fit to lensing geometry Koopmans & Treu Ap J 611, 739 (2004); Treu et al Ap J 640, 662 (2006) SLACS data suggests remarkable uniformity in isothermal mass profiles to z~1

  7. Mass-Dependent FP Evolution 142 GOODS z850<22.4 spheroidals: HST sizes, Keck dispersions If log RE = a log  + b SBE +  Effective mass ME 2RE / G For fixed slope, change in FP intercept ilog (M/L)I Treu et al Ap J 633, 174 (2005)

  8. Recent Growth in Low Mass Spheroidals High mass spheroidals (>1011.5 M) have <1% growth in young stars since z~1.2 Lower mass systems (< 1011 M) show 20-40% growth “age” • (M/L) - dynamical mass

  9. Caught in the Act: Blue Core Spheroidals 14/163 E+S0 have blue cores (defined s.t. rest frame (B-V) <-0.2) Similar confirmation from galaxies with strong H absorption

  10. v Dokkum & vd Marel (astro-ph/0609587) Treu et al Ap J 622, L5 (2005) Environmental Dependence of FP Evolution: I clusters field SDSS log  Only marginal trends seen with density (including SDSS): - mass-dependent growth is a galactic-scale phenomenon? - age differential (field vs cluster) ~ 0.4 Gyr @ z~0 (4%)

  11. Environmental Dependence of FP Evolution: II Coma Radial dependence of FP: 71 spheroidals in Cl0024+16 (z=0.40) Spheroidals in core are passively evolving since zF > 2 Outermost spheroids have younger stellar popn (t > 0.6 Gyr) Moran et al Ap J 634,977 (2005)

  12. Radial Trends in Spheroidals: Diagnostics of SF E+A • Sharp onset of [OII] emitters at RVIRIAL~1.5Mpc • Subsequently enhanced Balmer absorption (H) • Recently-arrived field galaxies interact with ICM in cluster environs • Model illustration: 200 Myr burst at RVIRIAL involving 1% burst by mass • “Environmental rejuvenation” as important as mass-dependent trends H + H [OII] R (Mpc) Field spheroidals undergo final activity during infall

  13. Effect of Environment on Disk Galaxies Rotation curves for matched sample of ~100 z~0.5 cluster & field spirals

  14. Disturbed Dynamics in Cluster Spirals Field Field Scatter in cluster TF relation is 2  that in field! Effect same in both V and K band so not due to M/L (or dust): kinematic origin (spatial dependence suggests harassment) Cluster Cluster MK MV Moran et al. 2006, ApJ submitted

  15. Spirals to S0s? GALEX Finds a `Smoking Gun’ NUV (2500Å) observed for 15ks (Cl0024+16) & 45ks (MS0451-03) Probes MS star formation on finer timescales (107-108 yrs) Cl0024 GALEX NUV - CFHT I GALEX NUV

  16. Two Complementary Clusters ICM mass density Clusters chosen to be very different in their X-ray properties MS0451-03 has 8 luminosity and 2 temperature of Cl0024+16 Influence of ICM on infalling galaxies will occur at different radii

  17. Passive Spirals: In Transition to S0s No optical emission (OII <5 Å) • lack of star formation Visible spiral structure • no major disruption to the structure of the galaxy (e.g. major merger) But strong FUV emission! Passive spirals caught in final decline in SFR in last 107-108 yr Sp E Moran et al Ap J 641, L97 (2006)

  18. Passive Spirals: Cl 0024 vs. MS 0451 Passive spirals less concentrated in MS0451 as expected for starvation Abundances  timescales sufficient for production of local S0s

  19. Can we dynamically separate Es and S0s to z~1? vROT, , e for: Cl0024/MS0451: 72 E/S0s z ~ 0.4-0.5 GOODS-N: 40 Field E/S0s 0.4<z<0.6 Watching Growth of S0s: Absorption Line Dynamics

  20. Dynamically-classified S0s: Find v/(1-) vs  is best discriminator Using this find: f(S0) ~205% at z~0.5 over 0.5< lg  < 2.5 At z=0 Dressler found f(S0)>40% in this  range: significant growth! Promising method..extending it to larger samples & higher z z~0.5 fSO

  21. Palomar+DEEP2 survey of mass assembly in field galaxies (Bundy et al astro-ph/0512465) Downsizing in Field Galaxies • Unique survey: DEEP2 spectroscopic z’s, IR-based stellar masses (KAB<21.5), 4 fields spanning 1.5 deg2, 8000g • Related morphological study in GOODS (Bundy et al Ap J 621, 625 2005) • Results • Little growth in massive quiescent galaxies; most evolution at lower mass: mirrored by decline in SF component • Detection of `quenching mass’ MQ above which SF ceases (as determined by any of morphology, color, OII) • Strong evolution in this threshold mass: MQ (1+z)3.5 • Little environmental density dependence in threshold mass

  22. Using rest-frame U-B color as a discriminant, a threshold stellar mass is apparent above which there is no SF • Mass threshold increases from ~1011 M at z~0.3 to ~1012M at z >1 • Stable from field-to-field (V/bin~2.106 Mpc3) • Little change for high mass quiescent galaxies over z<1 Downsizing & Star Formation Bundy et al (astro-ph/0512465)

  23. Evolution of Threshold Mass Transition mass Quenching mass Although SF cut-off can be defined in various ways, increase of mass with z is a robust result

  24. The `Declining Blues’ become the `Rising Reds’ Inconsistent with dominant assembly from dry mergers

  25. Testing Mass Assembly Dynamically For 142 GOODS-N morphologically-selected spheroidals we can directly compare IR-based stellar masses with dynamical ones (Bundy et al in prep) This allows us to estimate dynamical mass functions for a very large sample of spheroidals in GOODS

  26. Distinguish between downsizing in SF suppression and that in assembly: Construct time derivative of mass function: growth as a function of mass both dynamically and via stellar masses. Similar trend: low mass spheroidals grow much faster than high mass ones Downsizing in Mass Assembly Derivative

  27. Bulge Assembly V-I z HDF bulges ( °) are bluer & more diverse in their colors than most passively-evolving spheroidals (•) Ellis, Abraham & Dickinson ApJ 551, 111 2001

  28. Fundamental Plane of Intermediate z Bulges: I GOODS sample: N~60 bulges 0.2<z<0.6 HST photometric bulge/disk decomposition Keck: bulge stellar velocity dispersions, disk rotation MacArthur et al (in prep)

  29. Fundamental Plane of Intermediate z Bulges: II Bulges follow trends located for low mass Es: continued growth

  30. Dynamical data offers valuable insight into the processes that govern the assembly history of galaxies, complementing larger photometric analyses • Environmentally-driven processes are just as important as, and maybe independent of, galactic-scale feedback effects • Detailed case studies of clusters offer valuable insight into the processes involved: e.g. passive spirals & the continued production of S0s - a significant fraction of red light today • Data on `downsizing’ in field samples offers many puzzles for theorists: MQ (z), weak  dependence • Dynamical evidence suggests downsizing is not just related to suppression of SF but may extend also to assembly Conclusions

  31. The Fundamental Plane for Spheroidals: Empirical correlation between size, L and * • Considerably superior as a tracer of evolving mass/light ratio: • Dynamical mass: • no IMF dependence • Closer proxy for halo mass • Tough to measure: •  demands high s/n spectra • large samples difficult Dressler et al. 1987; Djorgovski & Davis 1987; Bender Burstein & Faber 1992; Jorgensen et al. 1996

  32. Combining Lensing & Stellar Dynamics ρ~r-γ On galactic scales, lensing and stellar dynamics provide complementary constraints on the mass distribution. In combination, therefore, they constrain the slope, , of the total mass distribution

  33. Remarkable Uniformity in Total Mass Profile

  34. Proper Account of Selection Biases local FP In flux limited sample, objects with low mass and high M/L are excluded at high z: dealt with full Monte-Carlo (Treu et al 2005b)

  35. Dynamics of GOODS-N Spirals

  36. Rotation Curves: Benefits of Long Integrations ACS viz Image DEIMOS Spectra 1hr Rotation Curve 10hr Rotation Curve 10hr z=0.633 1hr 10hr z=0.910 1hr 10hr z=0.938 1hr

  37. T- from COSMOS 2deg2 HST survey Capak et al (Ap J submitted)

  38. Stellar Mass Assembly by Morphological Type • No significant evolution in massive galaxies since z~1 (c.f. Fontana, Drory et al) • Modest decline with z in abundance of massive spheroidals, most change at lower mass (c.f. Treu et al) • Bulk of associated evolution is in massive Irrs 2dF Bundy et al (2005) Ap J 634,977 ( h = 1 )

  39. Downsizing Doesn’t Depend on Environment First Results - Color Is this consistent with merger-driven activity?

  40. Detailed Environmental Studies in Two Clusters Cl0024+16 (z=0.40) MS0451-03 (z=0.54) HST, GALEX, CFHT/Palomar BVRJK, MIPS to turn-around r~5 Mpc Morphologies for 4000 galaxies to F814W(Vega)=22.5 DEIMOS spectra of 3000 gals, 800 members (, vrot for ~240 members)I- Treu et al (2003) Ap J 591, 54 - morphology-density relation II- Kneib et al (2004) Ap J 598, 804 - DM mass profile III - Moran et al (2005) Ap J 634, 977 - environmental study of spheroidal FP IV- Moran et al (2006) Ap J 641, L79 - `passive spirals’ - a smoking gun V - Moran et al (submitted) - environmental study of spiral TF relation

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